| Summary: | The radiative capture reaction ¹⁶0(p,γ)¹⁷F has been studied theoretically using a two-body model to estimate the capture
cross sections.
The ¹⁶0(p,γ)¹⁷F reaction is a direct capture process at
low energies, which is of astrophysieal interest•because of its role
in the C-N-0 bi-cycle responsible for hydrogen burning in the larger
main sequence stars. The analysis done in this thesis involves a de-
tailed fitting of the ¹⁶0(p,p)¹⁶0 scattering data to search for the
parameters of a Saxon Woods potential with an energy dependent central well depth, which best describes the ¹⁶0+p interaction. The best set of parameters obtained is used to generate the initial continuum and bound state wave functions. The matrix elements of the electromagnetic
interaction hamiltonian are calculated and first order time dependent perturbation theory is used to- obtain the capture cross sections.
The results are compared with recent experimental data, observed
by T. Hall (1973), from 0.78 Mev to 2.3 Mev, which has a significantly higher accuracy than previous data that was available. The angular
distributions predicted by the theory agree satisfactorily with Hall's
data. The astrophysieal S-factor extrapolated to thermal energies has
the value 8.53 kev-barn at 10 kev, with an uncertainty of at least 5%„
Some of the methods used in the ¹⁶0(p,γ)¹⁷F calculations
are applied to a somewhat different capture reaction ⁶Li(p,γ)⁷Be, which involves interferences with resonance capture. This is included in an appendix; and because of the limited experimental data on this reaction, the results are much less conclusive. === Science, Faculty of === Physics and Astronomy, Department of === Graduate
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